Monte‐Carlo simulation of a possible correlation between the estimated luminosity distances and internal extinctions of type Ia supernovae     

L.G. Balzs  Zs. Hetesi  M. Korss 《Astronomische Nachrichten》2007,328(8):858-862

This paper describes a Monte Carlo simulation of type Ia supernova data. It was shown earlier that the data of SNe Ia might contain a possible correlation between the estimated luminosity distances and internal extinctions. This correlation was shown by different statistical investigations of the data. In order to remove observational biases (for example the effect of the detection limit of the observing instrument) and to test the reality of the effect found earlier we developed a simple routine which simulates extinction values, redshifts and absolute magnitudes for Ia supernovae. We pointed out that the correlation found earlier in the real data between the internal extinction and luminosity distance does not occur in the simulated sample. Furthermore, it became obvious that the detection limit of the observing devices used in supernova projects does not affect the far end of the redshift‐luminosity distance relationship of Ia supernovae. This result strengthens the earlier conclusions of the authors that SN Ia supernovae alone do not support the existence of dark energy. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Numerical investigation of the orbit of Interball‐1     

I. Nagy  B. rdi 《Astronomische Nachrichten》2007,328(8):793-796

We investigated the motion of the Earth's artificial satellite Interball‐1 by using a method suitable for the computation of large eccentricity orbits. Though the measured and the computed orbital elements differ from each other within the measured error bound, we found a slight tendency for secular decreasing in the semi‐major axis, caused probably by electromagnetic drag. We analysed the dominant role of the Moon in the variations of the orbital eccentricity, leading to zero perigee height and the end of the lifetime of the satellite. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

油页岩资源评价关键参数及其求取方法   总被引：6，自引：0，他引：6  

董清水  王立贤  于文斌  刘招君  张海龙  厚刚福 《吉林大学学报(地球科学版)》2006,36(6):899-903

资源评价关键环节之一就是评价参数标准的确定和求取。全国首次油页岩资源评价结果表明：油页岩质量评价关键参数主要有含油率（ω）、干燥基的灰分（A^g）、干燥基的低位发热量（Q^g_DW）及干燥基的全硫含量（S^g_Q）;油页岩资源量评价关键参数包括矿层可采厚度（H）、矿体有效面积（S）、矿体体重（D）、矿体资源类型等。不同参数的意义和评价标准不同,在表征单个工程控制点、块段油页岩体或单层油页岩等不同地质特征时,各参数的求取方法、计算公式有一定的差异性。进行油页岩资源评价时,应根据不同的目的选取不同的参数和计算方法。  相似文献   

The eSTAR network – agent architectures for astronomy     

A. Allan  T. Naylor  E. S. Saunders 《Astronomische Nachrichten》2006,327(8):767-770

The eSTAR Project uses intelligent agent technologies to carry out resource discovery, submit observation requests and analyze the reduced data returned from a meta‐network of robotic telescopes. Linking ground based telescopes with astronomical satellites, and using the emerging field of intelligent agent architectures to provide crucial autonomous decision making in software, the project has succeeded in combining data archives and research class telescopes, along with distributed computing nodes, to build an ad‐hoc peer‐to‐peer heterogeneous network of resources. We present the current operations paradigm of the eSTAR network and describe the direction in which the project intends to develop over the next few years. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The Gyldén‐type problem revisited: More refined analytical solutions     

A. Pal  D. elaru  V. Mioc  C. Cucu‐Dumitrescu 《Astronomische Nachrichten》2006,327(4):304-308

We resume and consistently extend our previous researches concerning the Gyldén‐type problem (a two‐body problem with time‐dependent equivalent gravitational parameter). To approach most of the concrete astronomical situations to be modelled in this way, we consider a periodic small perturbation. For the nonresonant case, we present a second‐order analytical solution. For the resonant case, we adopt the most realistic astronomical situation: only one dominant term of the Hamiltonian. In this case we point out a fundamental model of resonance, common to every resonant situation, and, moreover, identical to the first fundamental model of resonance . Considering the simplest model of periodic change of the equivalent gravitational parameter, we .nd that all possible resonances are con.ned to the first fundamental model. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

港口工程中非均质层状地基承载力计算方法     

袁凡凡  栾茂田  闫澍旺  孙万禾  毛明 《岩土力学》2006,27(7):1124-1128

在深水码头、防浪堤等大型港口工程建设中常常会遇到构筑物下覆地基由非均质的层状土构成的情况。对于这类非均质层状地基,我国港口工程地基规范推荐采用Hansen 61公式、Hansen 69公式和Sokolovskii数值解法3种方法计算地基的极限承载能力。然而,工程实践中由这3种方法计算得出的地基极限承载力数值往往有较大的差别。考虑到规范的继承性,基于牛顿迭代法,针对3个理论计算公式编制了计算程序,根据长江口深水治理二期工程地质实测资料,运用该计算程序对该地区地基的极限承载能力进行了计算比较。计算结果表明,对于非均质层状地基,在相同地质条件、相同荷载条件下Sokolovskii数值解法得到的承载力数值最大,Hansen 69公式得到的承载力数值最小。  相似文献   

土力学的现状及其数值分析方法中某些问题的讨论   总被引：8，自引：0，他引：8  

赵成刚 《岩土力学》2006,27(8):1361-1364

概括性地论述了土力学目前的状况,指出土力学仍然处于半理论、半经验的发展水平。论述了土力学数值分析方法在工程应用中存在的问题,并对如何正确地使用土力学的数值分析方法和改变土力学数值分析在工程应用中的不利状况进行了讨论。另外,就如何改善这种状况提出了一些措施。从这些讨论可以得到以下结论,土力学还处于发展的初期阶段,随着土力学的理论及其数值分析方法的不断发展,以及其使用经验的不断积累,计算土力学在工程实践中将会得到越来越多的应用,它必将成为岩土工程分析中的有力工具。  相似文献   

The Sloan Digital Sky Survey monitor telescope pipeline     

D.L. Tucker  S. Kent  M.W. Richmond  J. Annis  J.A. Smith  S.S. Allam  C.T. Rodgers  J.L. Stute  J.K. Adelman‐McCarthy  J. Brinkmann  M. Doi  D. Finkbeiner  M. Fukugita  J. Goldston  B. Greenway  J.E. Gunn  J.S. Hendry  D.W. Hogg  S.‐I. Ichikawa   . Ivezi&#x;  G.R. Knapp  H. Lampeitl  B.C. Lee  H. Lin  T.A. McKay  A. Merrelli  J.A. Munn  E.H. Neilsen  H.J. Newberg  G.T. Richards  D.J. Schlegel  C. Stoughton  A. Uomoto  B. Yanny 《Astronomische Nachrichten》2006,327(9):821-843

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi‐step process which involves data from three different telescopes: the 1.0‐m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5‐m Photometric Telescope (PT) at the Apache Point Observatory (APO), NewMexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5‐m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single‐CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0‐m and the PT). We also describe transformation equations that convert photometry on the USNO‐1.0m u ′g ′r ′i ′z ′ system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi‐automated PT factory, which runs MTPIPE in the day‐to‐day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS‐related projects, including the Southern u ′g ′r ′i ′z ′ Standard Star project, the u ′g ′r ′i ′z ′ Open Star Clusters project, and the SDSS extension (SDSS‐II). (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

TAOS – The Taiwanese‐American Occultation Survey     

M. J. Lehner  C. Alcock  T. Axelrod  F. Bianco  Y.‐I. Byun  W.‐P. Chen  K. H. Cook  R. Dave  I. de Pater  J. Giammarco  S.‐K. King  T. Lee  J. Lissauer  S. L. Marshall  S. Mondal  T. Nihei  J. Rice  M. Schwamb  A. Wang  S.‐Y. Wang  C.‐Y. Wen  Z.‐W. Zhang 《Astronomische Nachrichten》2006,327(8):814-817

The Taiwanese‐American Occultation Survey (TAOS) seeks to determine the number and size spectrum for small (∼3 km) bodies in the Kuiper Belt. This will be accomplished by searching for the brief occultations of bright stars (R ∼ 14) by these objects. We have designed and built a special purpose photometric monitoring system for this purpose. TAOS comprises four 50 cm telescopes, each equipped with a 2048 × 2048 pixel CCD camera, in a compact array located in the central highlands of Taiwan. TAOS will monitor up to 2 000 stars at 5 Hz. The system went into scientific operation in the autumn of 2005. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Piloting a network of small telescopes     

M. Fadavi  A. Verveer  J. Aymon  D. Merlin  K. Situ  C. Pennypackker  J. D. Biggs  G. White  A. Gould  G. Greenberg  V. Hoette  K. McCarron  K. Archer  F. Pino  M. Hibbs  M. Ford  J. Wetsch 《Astronomische Nachrichten》2006,327(8):811-813

The Pilot Small Telescope Network (PSTN) is a state‐of the art system of easily replicable and scalable hardware, software, servers, eXtensible Markup Language (XML) protocols, and network middleware connecting and developing a pilot array of robotic telescopes to one another and the user community. The PSTN is a developmental project that will allow growing access to these telescopes, and make available data to faculty, students and others in an environment of collaboration. The underlying goal of the PSTN is to broaden the quantity and quality of astronomical education and research, particularly with a focus on traditionally underserved populations. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献